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Accurate Absolute Magnitudes for Kuiper Belt Objects and Centaurs Icarus 179 (2005) 523–526 www.elsevier.com/locate/icarus Accurate absolute magnitudes for Kuiper belt objects and Centaurs W. Romanishin a,∗,1, S.C. Tegler b,1 a Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA b Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86011, USA Received 31 March 2005; revised 18 June 2005 Available online 15 August 2005 Abstract Accurate absolute optical magnitude values (HV and HR) for Kuiper belt objects (KBOs) and Centaurs are becoming increasingly impor- tant as observations in other wavelengths, particularly SIRTF thermal infrared measurements, become available for large samples of objects. We present accurate HV and HR values for 90 KBOs and Centaurs, based on our published optical photometry. We find that our HV values are in good agreement with those available from the European photometric survey of minor bodies in the outer Solar System. Comparison with HV values from the JPL Horizons database and the Minor Planet Center database shows that these sources are systematically brighter than ours by about 0.3 mag. 2005 Elsevier Inc. All rights reserved. Keywords: Centaurs; Kuiper belt objects; Trans-neptunian objects 1. Introduction magnitude is one of the most basic observable quantities of a minor Solar System body. There are now about 1000 cataloged minor outer So- Several groups are using infrared measurements of KBOs lar System bodies, with about 500 having been observed at and Centaurs, these being obtained with SIRTF, to measure more than one opposition. For the vast majority, nothing is the thermal emission properties of a subset of the population. known of their intrinsic physical properties. In 1995, we be- These observations should yield important new information gan a large and systematic program to obtain optical (BVR) on the sizes of these objects. Comparison of the infrared and colors and magnitudes for a sample of these objects. Our optical fluxes can yield the optical albedo. program has been aimed at obtaining accurate optical colors To obtain an accurate optical albedo from comparison and searching for correlations of color with various orbital of optical and infrared observations, an accurate optical ab- parameters (see, e.g., Tegler et al., 2003). In addition to opti- solute magnitude or flux value is required. Because of the cal colors, we have also obtained some information on light increasing importance of accurate values of optical parame- curves of individual objects (Romanishin and Tegler, 1999; ters, we present here such information for the objects for Romanishin et al., 2001). which we have published optical photometry. We also com- For all objects in our sample, we have measured accurate pare our derived HV values with those available from several V band magnitudes and V–R colors from at least one epoch. large databases of properties of minor Solar System bodies. These data can, of course, be used to derive an estimate of the absolute visual magnitudes (HV) of the objects. The HV 2. Absolute magnitudes * Corresponding author. Fax: +1 405 325 7557. E-mail address: [email protected] (W. Romanishin). We use the H , G formalism (Bowell et al., 1989) to derive 1 Observers at the Keck I, Bok, and Vatican Advanced Technology tele- the absolute visual magnitude (HV), which is the magnitude scopes. that would be observed in the V passband by an observer at 0019-1035/$ – see front matter 2005 Elsevier Inc. All rights reserved. doi:10.1016/j.icarus.2005.06.016 524 W. Romanishin, S.C. Tegler / Icarus 179 (2005) 523–526 a distance of 1 AU from an object that is 1 AU from the Sun, Table 1 at a phase angle of 0◦. HV and HR magnitudes We derive HV from the observed V magnitude, distances, Number Name Prov. Des. H H and phase angle: V R 2003 CO1 9.29 8.80 HV = V − 5log(r) 2001 XZ255 11.24 10.49 + 2.5log (1 − G)Φ1(α) + GΦ2(α) , (1) 2001 SQ73 9.24 8.78 2001 QX322 6.70 6.10 where V is the measured magnitude of the object in V band, 2001 KG77 8.62 8.18 r is the heliocentric distance (in AU) at the time of obser- 2001 KC77 7.23 6.67 vation, is the geocentric distance (in AU) at the time of 2001 FM194 7.91 7.47 observation, α is the phase angle (Sun–target–observer an- 2000 KK4 6.46 5.82 gle) at time of observation and 2000 FZ53 11.72 11.16 2000 FS53 7.88 7.17 1 Bi 2000 CR105 6.60 6.08 Φi(α) = exp −Ai tan α , (2) 2000 CQ105 6.29 5.85 2 2000 CF105 7.59 6.89 1999 TR11 8.63 7.88 where i = 1, 2, A1 = 3.33, B1 = 0.63, A2 = 1.87, B2 = 1999 HV11 7.47 6.88 1.22. 1999 HS11 6.88 6.16 We assume a G value of 0.15, which is the value most 1999 CF119 7.42 6.81 often adopted for this class of objects. Using observations 1998 WX24 6.79 6.09 = 1998 WV24 7.43 6.93 over a range of α, Buie and Bus (1992) derive G 0.16 for 1998 KS65 7.63 6.99 (5145) Pholus. Unfortunately, almost all of our observations 1998 FS144 7.17 6.60 of individual objects are made at a single epoch, so we can- 1997 SZ10 8.75 8.10 not constrain G values. 1997 QH4 7.44 6.77 Observed V magnitudes and observation dates were 1997 CV29 7.71 7.06 1997 CT29 7.19 6.44 taken from our published papers (Tegler and Romanishin, 1996 TS66 6.50 5.74 1998, 2000, 2003; Romanishin and Tegler, 1999; Tegler 1996 TQ66 7.69 6.99 et al., 2003). Distances (r and ) were derived from the 1996 TK66 6.75 6.12 JPL Horizons online database (Giorgini et al., 1996; http: 1996 RR20 7.20 6.49 //ssd.jpl.nasa.gov/horizons_doc.html). For objects with H 1996 RQ20 7.00 6.56 V 1995 HM5 8.29 7.88 listed in Romanishin and Tegler (1999),newHV values were 1994 TA 12.05 11.37 derived for consistency and also to use distances from orbits 1993 RO 8.92 8.41 with any improvements made since that paper. The new HV 1993 FW 7.09 6.46 values for these objects agree to within 0.01 mag with our 95626 2002 GZ32 7.24 6.82 previously published values. 88269 2001 KF77 10.52 9.79 87269 2000 OO67 9.82 9.10 Our derived HV values are listed in Table 1.Forthe 86047 1999 OY3 6.46 6.09 majority of the objects, we have observations taken only 85633 1998 KR65 7.10 6.43 during one night, or perhaps a few nights during one ob- 83982 2002 GO9 9.17 8.41 serving run. The information in this table is available online 82158 2001 FP185 6.38 5.80 at http://observatory.ou.edu/kbos.html. Our color survey is 82155 2001 FZ173 6.23 5.68 82075 2000 YW134 4.74 4.19 continuing, and we will update the online information as we 79360 1997 CS29 5.52 4.91 derive final magnitudes and colors for newly observed ob- 73480 2002 PN34 8.66 8.14 jects. For convenience we also list HR values in Table 1, 65489 2003 FX128 6.60 6.04 63252 2001 BL41 11.46 10.95 derived from the HV values and published V–R colors. 60621 2000 FE8 6.83 6.35 60608 2000 EE173 8.49 8.00 60458 2000 CM114 7.36 6.86 3. Comparison with other sources 55636 2002 TX300 3.47 3.11 54598 Bienor 2000 QC243 7.69 7.19 Another large photometric survey of minor outer Solar 52975 Cyllarus 1998 TF35 8.99 8.24 System bodies is available from a collaboration of a number 52872 Okyrhoe 1998 SG35 11.23 10.75 52747 1998 HM151 8.02 7.40 of observers using European Southern Observatory (ESO) 50000 Quaoar 2002 LM60 2.74 2.10 telescopes. They present HV values (Doressoundiram et al., 49036 Pelion 1998 QM107 10.54 10.02 2002) or HR values (Peixinho et al., 2004), which we con- 47171 1999 TC36 5.33 4.64 44594 1999 OX3 7.85 7.16 verted to HV values by adding their V–R color for each ob- ject. Ignoring a few objects in these lists with large (greater 42355 2002 CR46 7.65 7.13 (continued on next page) than 0.1) errors in HV, we find 30 objects in common with Absolute magnitudes of KBOs 525 Table 1 (continued) differences between the HV values listed in Table 1 and Number Name Prov. Des. HV HR those obtained from the other databases. The distribution of 38628 Huya 2000 EB173 5.03 4.43 magnitude differences are shown in Fig. 1. The average dif- 38084 1999 HB12 7.04 6.47 ference between JPL and ours (HV (JPL) − HV (ours)) is 33001 1997 CU29 6.68 6.02 −0.34 (s = 0.33). The average difference between MPC and 32929 1995 QY9 8.06 7.59 ours (HV (MPC) − HV (ours)) is −0.29 (s = 0.34). Thus, 32532 Thereus 2001 PT13 9.32 8.85 these HV magnitudes are significantly brighter than ours. 31824 Elatus 1999 UG5 10.49 9.82 29981 1999 TD10 9.06 8.59 To find the origin of these systematic offsets in HV val- 26375 1999 DE9 5.20 4.62 ues, one would have to carefully review the input magni- 26308 1998 SM165 6.13 5.38 tudes into the databases for each object.
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